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Chromospheric Activity in G and K Main-Sequence Stars, and What It Tells Us about Stellar Dynamos
For main-sequence G and K stars we study again the empirical relationsbetween the periods of the activity cycles, Pcyc, and therotational periods, prot. We use the high-quality dataselected by Brandenburg, Saar, and Turpin. As found by those authors``the Pcyc increase proportional to the prot,along two distinctly different sequences,'' the active ``A'' sequence,and the inactive ``'I'' sequence with cooler and more slowly rotatingstars. It is found here that along each sequence the number of rotationperiods per activity cycle is nearly the same, but the numbers aredifferent for the different sequences, indicating that probablydifferent kinds of dynamos are working for the stars on the differentsequences. The transition from one sequence to the other occurs at arotation period of 21 days. The rotation periods then increase abruptlyby about a factor of 2 for the cooler stars. We suggest that thisindicates abruptly increased deep mixing. Along the I sequence theoverall dependence of the Ca II emission line fluxes, F(Ca II), onrotation and Teff is consistent with F(CaII)~T4effp-4/3rot. For theA-sequence stars the dependence of F(Ca II) on rotation seems to bestronger than for the I-sequence stars.
| A HIPPARCOS Census of the Nearby OB Associations
A comprehensive census of the stellar content of the OB associationswithin 1 kpc from the Sun is presented, based on Hipparcos positions,proper motions, and parallaxes. It is a key part of a long-term projectto study the formation, structure, and evolution of nearby young stellargroups and related star-forming regions. OB associations are unbound``moving groups,'' which can be detected kinematically because of theirsmall internal velocity dispersion. The nearby associations have a largeextent on the sky, which traditionally has limited astrometricmembership determination to bright stars (V<~6 mag), with spectraltypes earlier than ~B5. The Hipparcos measurements allow a majorimprovement in this situation. Moving groups are identified in theHipparcos Catalog by combining de Bruijne's refurbished convergent pointmethod with the ``Spaghetti method'' of Hoogerwerf & Aguilar.Astrometric members are listed for 12 young stellar groups, out to adistance of ~650 pc. These are the three subgroups Upper Scorpius, UpperCentaurus Lupus, and Lower Centaurus Crux of Sco OB2, as well as VelOB2, Tr 10, Col 121, Per OB2, alpha Persei (Per OB3), Cas-Tau, Lac OB1,Cep OB2, and a new group in Cepheus, designated as Cep OB6. Theselection procedure corrects the list of previously known astrometricand photometric B- and A-type members in these groups and identifiesmany new members, including a significant number of F stars, as well asevolved stars, e.g., the Wolf-Rayet stars gamma^2 Vel (WR 11) in Vel OB2and EZ CMa (WR 6) in Col 121, and the classical Cepheid delta Cep in CepOB6. Membership probabilities are given for all selected stars. MonteCarlo simulations are used to estimate the expected number of interloperfield stars. In the nearest associations, notably in Sco OB2, thelater-type members include T Tauri objects and other stars in the finalpre-main-sequence phase. This provides a firm link between the classicalhigh-mass stellar content and ongoing low-mass star formation. Detailedstudies of these 12 groups, and their relation to the surroundinginterstellar medium, will be presented elsewhere. Astrometric evidencefor moving groups in the fields of R CrA, CMa OB1, Mon OB1, Ori OB1, CamOB1, Cep OB3, Cep OB4, Cyg OB4, Cyg OB7, and Sct OB2, is inconclusive.OB associations do exist in many of these regions, but they are eitherat distances beyond ~500 pc where the Hipparcos parallaxes are oflimited use, or they have unfavorable kinematics, so that the groupproper motion does not distinguish it from the field stars in theGalactic disk. The mean distances of the well-established groups aresystematically smaller than the pre-Hipparcos photometric estimates.While part of this may be caused by the improved membership lists, arecalibration of the upper main sequence in the Hertzsprung-Russelldiagram may be called for. The mean motions display a systematicpattern, which is discussed in relation to the Gould Belt. Six of the 12detected moving groups do not appear in the classical list of nearby OBassociations. This is sometimes caused by the absence of O stars, but inother cases a previously known open cluster turns out to be (part of) anextended OB association. The number of unbound young stellar groups inthe solar neighborhood may be significantly larger than thoughtpreviously.
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Membre dels grups següents:
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Dades d'Observació i Astrometria
| Constel·lació: | Vela |
| Ascensió Recta: | 09h05m40.19s |
| Declinació: | -47°32'22.8" |
| Magnitud Aparent: | 9.091 |
| Moviment propi RA: | -11.6 |
| Moviment propi Dec: | 7.9 |
| B-T magnitude: | 9.124 |
| V-T magnitude: | 9.094 |
Catàlegs i designacions:
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